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Portions of the Kepler K2 Short Cadence light curve of the dwarf nova (DN) TWVir at quiescence are investigated using light curve modeling. The light curvewas separated into 24 sections, each with a data length of $\sim\,$0.93\,d,comprising 4 sections before and 20 after a superoutburst (SO). Due to themorphological differences, the quiescent orbital modulation is classified intothree types. Using a fixed disk radius and the two component stellarparameters, all 24 synthetic disk models from the sections show a consistentconfiguration, consisting of a disk and two hotspots: one at the vertical sideof the edge of the disk and the other one on the surface of the disk. Beforethe SO, the disk and a ringlike surface-hotspot are suddenly enhanced,triggering a precursor and then SO. At the end of the quiescent periodfollowing the SO and before the first normal outburst, the edge-hotspot becomeshotter, while the surface-hotspot switches into a ``coolspot" with a coverageof nearly one-half of the disk surface. During quiescence, the surface-hotspotis always located at the outer part of the disk with a constant radial width. Aflat radial temperature distribution of the disk is found and appears flatterwhen approaching the outburst. Like many U\,Gem-type DN with orbital periods of3-5\,hr, the mass transfer rate is significantly lower than the predictions ofthe standard/revised models of CV evolution.

Evolution of the Quiescent Disk surrounding a Superoutburst of the Dwarf Nova TW Virginis